Issue |
A&A
Volume 559, November 2013
|
|
---|---|---|
Article Number | A59 | |
Number of page(s) | 12 | |
Section | Galactic structure, stellar clusters and populations | |
DOI | https://doi.org/10.1051/0004-6361/201322085 | |
Published online | 14 November 2013 |
Chemical gradients in the Milky Way from the RAVE data
I. Dwarf stars
1
Astronomisches Rechen-Institut, Zentrum für Astronomie der
Universität Heidelberg, Mönchhofstr. 12-14, 69120
Heidelberg,
Germany
e-mail:
corrado@ari.uni-heidelberg.de
2
Leibniz Institut für Astrophysik Potsdam (AIP),
An der Sternwarte 16,
14482
Potsdam,
Germany
3
Observatoire de Strasbourg, Université de
Strasbourg, CNRS 11 rue de
l’Université, 67000
Strasbourg,
France
4
Sydney Institute for Astronomy, School of Physics A28, University
of Sydney, NSW
2006, Australia
5
Institute of Astronomy, University of Cambridge,
Madingley Road, Cambridge
CB3 0HA,
UK
6
Jeremiah Horrocks Institute, University of Central
Lancashire, Preston,
PR1 2HE,
UK
7
Monash Centre for Astrophysics, School of Mathematical Sciences,
Monash University, Clayton, VIC,
3800,
Australia
8
INAF Osservatorio Astronomico di Padova,
via dell’Osservatorio 8,
36012
Asiago,
Italy
9
Department of Physics and Astronomy, Padova
University, Vicolo
dell’Osservatorio 2, 35122
Padova,
Italy
10
University of Victoria, PO Box 3055, Station CSC, Victoria, BC
V8W 3P6,
Canada
11
Department of Physics & Astronomy, Macquarie
University, NSW
2109
Sydney,
Australia
12
Research Centre for Astronomy, Astrophysics and Astrophotonics,
Macquarie University, NSW
2109
Sydney,
Australia
13
Australian Astronomical Observatory, PO Box 915, NSW 1670
North Ryde,
Australia
14
Mullard Space Science Laboratory, University College
London, Holmbury St
Mary, Dorking,
RH5 6NT,
UK
15
Department of Physics and Astronomy, Johns Hopkins
University, 3400 North Charles
Street, Baltimore,
MD
21218,
USA
16
Faculty of Mathematics and Physics, University of
Ljubljana, Jadranska
19, 1000
Ljubljana,
Slovenia
17
Center of Excellence SPACE-SI, Askerceva cesta 12, 1000
Ljubljana,
Slovenia
Received:
14
June
2013
Accepted:
27
August
2013
Aims. We aim at measuring the chemical gradients of the elements Mg, Al, Si, and Fe along the Galactic radius to provide new constraints on the chemical evolution models of the Galaxy and Galaxy models such as the Besançon model. Thanks to the large number of stars of our RAVE sample we can study how the gradients vary as function of the distance from the Galactic plane.
Methods. We analysed three different samples selected from three independent datasets: a sample of 19 962 dwarf stars selected from the RAVE database, a sample of 10 616 dwarf stars selected from the Geneva-Copenhagen Survey (GCS) dataset, and a mock sample (equivalent to the RAVE sample) created by using the GALAXIA code, which is based on the Besançon model. The three samples were analysed by using the very same method for comparison purposes. We integrated the Galactic orbits and obtained the guiding radii (Rg) and the maximum distances from the Galactic plane reached by the stars along their orbits (Zmax). We measured the chemical gradients as functions of Rg at different Zmax.
Results. We found that the chemical gradients of the RAVE and GCS samples are negative and show consistent trends, although they are not equal: at Zmax< 0.4 kpc and 4.5 <Rg(kpc) < 9.5, the iron gradient for the RAVE sample is d [Fe/H] /dRg = −0.065 dex kpc-1, whereas for the GCS sample it is d [Fe/H] /dRg = −0.043 dex kpc-1 with internal errors of ±0.002 and ±0.004 dex kpc-1, respectively. The gradients of the RAVE and GCS samples become flatter at larger Zmax. Conversely, the mock sample has a positive iron gradient of d [Fe/H] /dRg = +0.053 ± 0.003 dex kpc-1 at Zmax< 0.4 kpc and remains positive at any Zmax. These positive and unrealistic values originate from the lack of correlation between metallicity and tangential velocity in the Besançon model. In addition, the low metallicity and asymmetric drift of the thick disc causes a shift of the stars towards lower Rg and metallicity which, together with the thin-disc stars with a higher metallicity and Rg, generates a fictitious positive gradient of the full sample. The flatter gradient at larger Zmax found in the RAVE and the GCS samples may therefore be due to the superposition of thin- and thick-disc stars, which mimicks a flatter or positive gradient. This does not exclude the possibility that the thick disc has no chemical gradient. The discrepancies between the observational samples and the mock sample can be reduced by i) decreasing the density; ii) decreasing the vertical velocity; and iii) increasing the metallicity of the thick disc in the Besançon model.
Key words: Galaxy: abundances / Galaxy: evolution / Galaxy: structure / Galaxy: kinematics and dynamics
© ESO, 2013
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